Date of Birth:1986-12-07
Date of Employment:2014-01-01
Business Address:Room 512
Geophysics Building
Administrative Position:None

Xiao Zhiyong

Associate professor


The Last Update Time:..

Education Level:Doctoral Degree in Education
Alma Mater:China University of Geosciences
Professional Title:Associate professor
tshonorcengYoung Talent Program, China Association For Science and Technology
2017 AOGS Gistinguished Young Scholar Other Post:None
School/Department:School of Earth Sciences
Academic Titles:None

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Personal Information

Research Interests:Remote sensing, Planetary surface processes; Earth Impact craters Key words:Impact cratering, Crater chronology, Earth Impact Craters, Tektites, Dark spots, Mercury, Moon_____________________________________________________________________________Courses:Structural Geology, Planetary Surface Processes————————————————————————————————Recruit graduate students direction:Currently, my researches are focued on the three following subjects.1) Impact craters on planetary surfaces [NSFC supported]As the most important geologic process on planetary bodies including the Earth, impact cratering is a definite beauty because of its enourmous energy and scale. The physical processes related with impact cratering are amazing and intriguing. Thinking about building the Dabie Mountain has cost how many millions of years, but forming a even larger mountain belt just takes less than 5 minutes by impact cratering. Rock vaporization, melting, strong metamorphism, and deformation all literally occur in less than a blink during impact cratering.My target is to understand details about the physical processes related with impact cratering. Besides some numerical modelling work using the iSALE hydrocode (, most of my researches are related with the morphology and topography of impact craters on various bodies. Since impact velocity, target properties, surface gravity are different on difrerent planetary bodies, the morphological and topography differences of impact craters on different bodies reveal the contribution of different factors in the cratering process. These observations are the ONLY ground truth, which provides direct guildlines for impact modeling and simulations.Here are some projects that I am now studying: (1) Controlling factors on ejection angles: secondary craters on continuous secondaries facies typically have very irregular shapes on all planetary bodies. However, many impact craters on Mercury (Xiao et al., 2014) and three impact basins on the Moon (Zhou et al., 2015) have abnormally circular secondaries, such as the ones shown in the image below. What is the reason for the abnormally larger ejection angles? My students and me are now collecting such craters on Mercury and other bodie. We will quantitatively constrain this special morphology and distribution characteristics using ArcMap, USGS ISIS, ENVI, and other image processing softwares. Together with topography, gravity, crustal thickness, reflectance spectra data, we will try to decode the major factor controlling ejection angles. (2) Formation mechanism of central pits in impact craters: Central pits are frequently observed on Mars and icy satelliates, therefore these topography depressions are attributed to the effect of target/projectile properties on crater formation. However, we recently found impact craters on both Mercury and the Moon have such features (see the image below), and they are not even smaller compared with those on Mars and icy satelliates. What are their formation mechanism? We are studying the morphology and size of such features on different bodies. Together with their background geology, we will try to constrain the fundamental process that has formed the depression. (3) Emplacement of crater ejecta: impact cratering moblizes a lot materials: The major events during the excavation stage are well constrained (see the image below), but they are still too rough to explain detailed observations (e.g., crater rays). The morphology and size of different crater exterior deposits are the key to understand this process. Studying crater ejecta on different airless bodies such as Mercury, the Moon, and 4Vesta would reveal the emplacement dynamics and sequence of ejecta; considering those on Mars and Venus would further shade light on the interation of atmosphere and high-velocity ejecta.Students who are interested on the above three projects should have at least one of...

Education Background
  • 2010.9 -- 2012.9
    University of Arizona , geology  , 博士学位 , Faculty of Higher Institutions
  • 2008.9 -- 2013.12
    中国地质大学(武汉) , geology  , 博士学位 , Faculty of Higher Institutions
  • 2006.3 -- 2008.6
    华中科技大学 , English  , 学士学位 , Double Degree Programs (Undergraduate)
  • 2004.9 -- 2008.6
    中国地质大学(武汉) , Computer science and technology  , Bachelor's Degree in Engineering , Editor
Work Experience
  • 2015.10 -- 2017.10
    University of Oslo , Centre for Earth Evolution and Dynamics , 无 , Guest Researcher , 离职
  • 2014.10 -- 2015.10
    University of Oslo , Centre for Earth Evolution and Dynamics , 无 , Postdoc Researcher , 离职
Social Affiliations
No content
Research Focus
  • Impact cratering processes, Earth impact craters,Crater chronology, tektites, and other planetary surface processes

Research Group
  • 李周波
  • 周琦深
  • 张世晖
  • 张鹏飞
  • 闫政旭
  • 付茹
  • 马金良
  • 周传波
  • 李周波
  • 周琦深